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Radial velocities of clusters between the Magellanic Clouds

Published online by Cambridge University Press:  19 July 2016

S. Demers ,
L. Grondin† ,
M. J. Irwin  and
W.E. Kunkel
S. Demers
Affiliation:
Department of Physics, Université de Montréal, Montreal, Canada
L. Grondin†
Affiliation:
Department of Physics, Université de Montréal, Montreal, Canada
M. J. Irwin
Affiliation:
Institute of Astronomy, Cambridge University, Cambridge, England
W.E. Kunkel
Affiliation:
The Observatories of the Carnegie Institution of Washington, La Serena, Chile

Abstract

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Radial velocities of 20 stars members of young clusters and associations located in the inter-Cloud region within 2h < R.A. < 5h tend to be lower than the HI velocities in the same direction. The stellar velocities do not show a pronounced velocity gradiant as observed for the HI from the SMC to the LMC. This suggests that the stellar components belong to the SMC wing. Our photometry and spectroscopy support the view that one of the stars at 4h20m is a foreground HB star.

Type
The LMC-SMC-Galaxy System
Information
Symposium - International Astronomical Union , Volume 148: The Magellanic Clouds , 1991 , pp. 473 - 474
Copyright
Copyright © Kluwer 1991 

References

Greenstein, J.L. and Sargent, A.I. (1974), Astrophys. J. Suppl. 28, 157.CrossRefGoogle Scholar
Irwin, M.J., Demers, S. and Kunkel, W.E. (1990), Astron. J. 99, 191.CrossRefGoogle Scholar
McGee, R.X. and Newton, L.M. (1986), Proc. Astron. Soc. Australia 6, 471.Google Scholar